Data Set Information
DATA_SET_NAME VOYAGER 1&2 JUPITER BRIGHTNESS NORTH/SOUTH MAP SET V1.0
DATA_SET_ID VG1/VG2-J-UVS-5-BRIGHTNESS-N/S-MAPS-V1.0
NSSDC_DATA_SET_ID NULL
DATA_SET_TERSE_DESCRIPTION VOYAGER 1&2 JUPITER BRIGHTNESS NORTH/SOUTH MAP SET V1.0
DATA_SET_DESCRIPTION
Data Set Overview
    =================
      This data set contains Voyager 1 and 2 measurements of the
      brightness of Jupiter at H Lyman alpha and in the H2 Lyman and
      Werner bands shortward of H Lyman alpha.  Pointing has been
      corrected by the C-Smithing process, and these data were derived
      from the pre-encounter North-South Map sequences.  In this
      sequence, the UVS field of view was located near the central
      meridian of the planet.  The field of view stepped slowly from
      north to south, and then rapidly repositioned to the north.
      These scans were repeated until all Jovian longitudes had been
      sampled.  Coverage in longitude was not continuous in time.
      Rather, some longitude ranges were covered on the preceding or
      following rotation of Jupiter.
 
      The brightnesses represent integrals over the appropriate
      passband that have been computed from the full spectrum.  The
      spectra were binned by Flight Data System (FDS) count, so that
      each record contains the data from one 48-second frame.
      Because the motion of the scan platform was synchronized with
      FDS count, each record corresponds to a single pointing
      position on Jupiter.  The first two spectra of each FDS count
      have been excluded, because the scan platform was moving during
      those times.  In some cases (e.g.  during the flyback slews to
      prepare for another N/S scan) all spectra were flagged with bad
      pointing status, and no spectra appear in the output bin.  The
      data in each time bin was normalized by dividing by the number
      of spectra binned, so that the spectra represent counts per
      3.84 second interval (the integration time in the GS-3 data
      mode used for most of the encounter sequences).  The final
      processing step in the spectral analysis stage was a correction
      for fixed pattern noise (flat fielding).
 
      The brightnesses were computed by summing over the appropriate
      wavelength channels.  These are:
 
                             Voyager 1
          Emission          channel range      wavelength range (A)
            H2 bands          43 - 58             924 - 1072
            H Lyman alpha     70 - 78            1174 - 1257
 
                             Voyager 2
          Emission          channel range      wavelength range (A)
            H2 bands          45 - 60             921 - 1069
            H Lyman alpha     72 - 80            1171 - 1254
 
      The brightnesses were corrected for dark counts, which arise
      mainly from the Jovian radiation environment.  Because the
      radiation-induced dark count rate depends rather sensitively on
      the magnetic latitude of the spacecraft, and hence on time,
      this correction is made on a spectrum-by-spectrum basis.  For
      the H Lyman alpha emission, the procedure also compensates
      approximately for H2 band emissions that fall within the H
      Lyman alpha channel range.  This correction procedure consists
      of subtracting the sum over suitably chosen background
      channels.  These background channels are:
 
                             Voyager 1
          Emission          channel range      wavelength range (A)
            H2 bands          23 - 38             739 -  887
            H Lyman alpha     58 - 66            1063 - 1146
 
                             Voyager 2
          Emission          channel range      wavelength range
            H2 bands          25 - 40             736 -  884
            H Lyman alpha     60 - 68            1060 - 1143
 
      Each record contains pointing information that consists of the
      latitude and System III longitude of the two ends of the slit
      (P2 and P8 points) and the center of the slit (P5 point)
      projected on Jupiter.  In addition, each point has associated
      with it a status flag.  A minus (-) means that the line of
      sight for the specified point intersects the planet.  A plus
      (+) means that the line of sight is off the planet.  In the
      latter case, the latitude and longitude refer to the point on
      the planet that is under the point of closest approach to the
      planet of the line of sight.
 
      Each logical record corresponds to one FDS count, and consists
      of three lines in the data file.  The quantities on each line
      are:
 
          first line:  Spacecraft Event Time, FDS count, S/C to
                       Jupiter range.
 
         second line:  P2 latitude, P2 longitude, P5 latitude,
                       P5 longitude, P8 latitude, P8 longitude,
                       P2 status, P5 status, P8 status
 
          third line:  H Lyman alpha counts, H2 band counts.
 
      For a detailed description of the data set contents, see
      [SANDELETAL1979; DESSLERETAL1981; and BROADFOOTETAL1981].
 
 
    Parameters
    ==========
 
      Voyager 1 Encounter Times
      -------------------------
        Start Time  : 1979-061/19:58:00 (1979-03-02)
        Stop Time   : 1979-062/09:20:57 (1979-03-03)
 
 
      Voyager 2 Encounter Times
      -------------------------
        Start Time  : 1979-187/11:52:11 (1979-07-07)
        Stop Time   : 1979-188/05:16:05 (1979-07-08)
 
 
      Data Set Parameter 'H LYMAN ALPHA BRIGHTNESS'
      ---------------------------------------------
        Data Set Parameter Name        : H LYMAN ALPHA BRIGHTNESS
        Data Set Parameter Unit        : COUNTS
        Sampling Parameter Name        : TIME
        Sampling Parameter Unit        : SECOND
        Minimum Sampling Parameter     : 48
        Maximum Sampling Parameter     : 48
        Sampling Parameter Resolution  : 48
        Sampling Parameter Interval    : 48
        Minimum Available Sampling Int : 48
        Noise Level                    : UNK
 
 
      Data Set Parameter 'H2 BAND BRIGHTNESS'
      ---------------------------------------
        Data Set Parameter Name        : H2 BAND BRIGHTNESS
        Data Set Parameter Unit        : COUNTS
        Sampling Parameter Name        : TIME
        Sampling Parameter Unit        : SECOND
        Minimum Sampling Parameter     : 48
        Maximum Sampling Parameter     : 48
        Sampling Parameter Resolution  : 48
        Sampling Parameter Interval    : 48
        Minimum Available Sampling Int : 48
        Noise Level                    : UNK
DATA_SET_RELEASE_DATE 1995-10-08T00:00:00.000Z
START_TIME 1979-03-02T07:58:00.000Z
STOP_TIME 1979-07-07T05:16:05.000Z
MISSION_NAME COMET SL9/JUPITER COLLISION
VOYAGER
MISSION_START_DATE 1993-01-01T12:00:00.000Z
1972-07-01T12:00:00.000Z
MISSION_STOP_DATE 1996-01-01T12:00:00.000Z
N/A (ongoing)
TARGET_NAME JUPITER
TARGET_TYPE PLANET
INSTRUMENT_HOST_ID VG1
VG2
INSTRUMENT_NAME ULTRAVIOLET SPECTROMETER
ULTRAVIOLET SPECTROMETER
INSTRUMENT_ID UVS
UVS
INSTRUMENT_TYPE ULTRAVIOLET SPECTROMETER
ULTRAVIOLET SPECTROMETER
NODE_NAME Planetary Atmospheres
ARCHIVE_STATUS ARCHIVED
CONFIDENCE_LEVEL_NOTE
Confidence Level Overview
    =========================
      Bad spectra resulting from telemetry noise and other effects
      have been omitted from this data set.  Spectra acquired when
      the scan platform was in motion have also been omitted to
      reduce spatial smearing as much as possible.  Some spatial
      smearing due to s/c limit cycle motions is unavoidable.
 
      The pointing information for the data set was derived by the
      C-Smithing (image navigation) process at JPL.  This improved
      pointing is believed to be the most accurate pointing
      information available.
CITATION_DESCRIPTION Citation TBD
ABSTRACT_TEXT This data set contains Voyager 1 and 2 measurements of the brightness of Jupiter at H Lyman alpha and in the H2 Lyman and Werner bands shortward of H Lyman alpha. Pointing has been corrected by the C-Smithing process, and these data were derived from the pre-encounter North-South Map sequences. In this sequence, the UVS field of view was located near the central meridian of the planet. The field of view stepped slowly from north to south, and then rapidly repositioned to the north. These scans were repeated until all Jovian longitudes had been sampled. Coverage in longitude was not continuous in time. Rather, some longitude ranges were covered on the preceding or following rotation of Jupiter.
PRODUCER_FULL_NAME DR. BILL R. SANDEL
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